Post-Periastron ASCA Observation of the PSR B1259-63 System
著者
和文:
Hirayama, M.,
Nagase, F.,
Tavani, M.,
Kaspi, V. M.,
河合 誠之,
Arons, J..
英文:
Hirayama, M.,
Nagase, F.,
Tavani, M.,
Kaspi, V. M.,
Kawai, N.,
Arons, J..
言語
English
掲載誌/書名
和文:
英文:
Publications of the Astronomical Society of Japan
巻, 号, ページ
Vol. 48
pp. 833-840
出版年月
1996年12月
出版者
和文:
英文:
会議名称
和文:
英文:
開催地
和文:
英文:
アブストラクト
We report on the results of a post-periastron ASCA observation of the PSR B1259-63 system, containing a 48 ms pulsar orbiting a Be star in an eccentric 3.4 yr orbit. The ASCA observation was carried out on 1994 February 28 when the radio pulsar was again visible after a prolonged 40-day radio eclipse near to periastron. The source was clearly detected with an X-ray luminosity (1--10 keV) L_X of ( 1.03 +/- 0.09 ) times 10(34) \ (d/2 kpc)(2) erg s(-1) , where d is the pulsar's distance. The X-ray spectrum is well-represented by a single power-law model of the photon index, alpha = 1.61 +/- 0.06, and a small photoelectric absorption, N_H = (5.6 +/- 0.6) times 10(21) cm(-2) . No significant X-ray pulsations were detected, and the upper limit for the pulsed component was estimated to be 15% of the total X-ray flux, assuming sinusoidal modulation. The characteristics of the X-ray emission detected on 1994 February 28 are similar to those detected by ASCA near periastron when the pulsed radio emission from PSR B1259-63 was eclipsed. Our results strongly favor a non-thermal model of X-ray emission driven by synchrotron radiation from relativistic shocked particles in the pulsar wind interacting with the outflow from the Be star companion.
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